Second Term Test is coming up Nov 1. Phys 1830: Lecture 19 (Image unknown origin) Second Term Test is coming up Nov 1. Review is now posted on our class website. Previous Class: Visualization: Computer Simulations Planetary Systems This Class: Solar System Solar System Formation Next Class: Solar System Formation continued Tour of the Solar System ALL NOTES COPYRIGHT JAYANNE ENGLISH

Public Talk March 13th – Neil deGrasse Tyson DREAM BIG! (A Student Life event) Email me today with your interests or visit me Monday to discuss. Image-making workshop  exhibition in “campo” produce a display of space milestones – needs a coordinator and volunteers

Planetary Systems Simulations start with disks filled with gas and dust. Observations motivate this initial configuration.

Planetary Systems & Disks -- Solar System: Looking towards the Sun Looking towards Jupiter The orbits of the 8 classical planets also indicate that our solar system evolved out of a disk. The planets’ orbits lay in a narrow plane. Mercury deviates the largest (with only a 7 degree tilt). They all orbit in the same direction. Looking from the earth in 2 different directions in the solar system. The planets are distributed in a disk. As seen from above the earth’s north pole they all orbit counterclockwise. This is from a nifty simulator from NASA. http://space.jpl.nasa.gov/

Assumption that planets form in disks was motivated by observations. Planetary Systems Eagle Nebula (M16) The length of the pillar on the left is about the same distance between our sun and the nearest stars. Assumption that planets form in disks was motivated by observations. Is the assumption that the disk is initially very gaseous a good one?

Molecular Cloud with “fingers” protruding. Planetary Systems Molecular clouds have molecules of hydrogen (2 H atoms share their electrons), carbon monoxide (CO), for example. Molecular Cloud with “fingers” protruding. Evaporating Gaseous Globules = EGGs at finger tips. Each about the size of our solar system.

Planetary Systems: Bok Globules in Carina Nebula Surrounding molecular gas cloud photoevaporates leaving denser globules of rotating gas. Material in a globule falls towards the centre via gravity. Simultaneously, due to conservation of angular momentum, a disk consisting mainly of gas and dust forms --> proplyds. Photoevaporation: the process in which a cloud is dispersed by the radiation from a nearby hot star. E.g. the bonds of molecules are broken as the photons are absorbed. The resultant atoms of gas also become ionized. Motion of globule can be due to turbulence in the gas cloud and other factors. Think of a skater turning, her skirt goes up like a tutu around her waist. Recall for angular momentum, as the radius decreases the disk is going to spin faster!

The central condensation will become a star. Planetary Systems Animation from Swinburne University, Centre for Astronomy and Supercomputing. Assumption that gas dominates the initial conditions is also founded on observations. The central condensation will become a star.

Planetary System Formation - Observations: Orion is an example of a dusty, gas cloud forming planetary systems. Distance is 1,500 ly (460 parsecs). Proplyds and Bok Globules inform the simulations of star and planet formation.

Visualizations: Simulations of Planetary Systems Observations Animation based on Simulation Observations of a planetary system with a ring and planets can be explained by a simulation. Planetary disk simulations use: gravity between particles, gravity between particles and the protostar, hydrodynamical forces Note that the planets have cleared their orbits in the simulations.

Visualizations: Simulations Two assumptions for modelling the formation of planets are: A cloud composed of rocks collapses. This forms a disk. (The biggest rocks are the planets.) A cloud composed mainly of gas collapses. This forms a disk. (Planets form within this disk.) Chunks of gas tear off from molecular clouds. Photo-evaporation exposes the planets buried inside these Bok Globules.

Extra-solar planets == Exoplanets More on this after we study our own Solar System

The models also have to match features of our own Solar System. The assumptions in the models of the formation of planetary systems are reasonable since supported by observations of other “solar systems”: Gas dominates Disks form The models also have to match features of our own Solar System. Why do all the planets orbit in a plane? Why do they orbit in the same direction? Why are some planets gaseous and others not?

Solar System Overview: Planet Definitions Classical Planet Orbits the sun. Massive enough that is own gravity has caused its shape to be nearly spherical. It has “cleared the neighbourhood” around its orbit of other bodies. i.e. either by colliding with (sweeping up) the debris in the disk or by gravitationally kicking the debris out of its path (slingshot effect). This leaves us with 8 planets.

Solar System Overview: Planet Definitions Dwarf Planet Orbits the sun. Massive enough that is own gravity has caused its shape to be spherical. Is not a satellite of another body. (Has not cleared its neighbourhood.) Exact wording is at http://www.iau.org/public_press/news/detail/iau0602/ . See International Astronomical Union Resolution 5A. Examples: Pluto Eris (1.3 * Pluto’s mass) Ceres (in the asteroid belt) Objects at Neptune and beyond are called Trans-Neptune Objects (TNO) and those TNO that are similar to Pluto are called plutoids.

Solar System Overview: What does the class already know about the classical planets? Divide up into 8 teams – one team per planet. A note-taker per team. 2 judges. Can use textbooks, computers (if you downloaded stuff), pictures, and, most importantly, humour! Presentations are a maximum of 5 min. When other people are presenting, take notes since we don’t have a textbook.

revolve & rotate in the same direction as other planets? Solar System Overview: What does the class already know about the classical planets? For each planet: revolve & rotate in the same direction as other planets? primarily composed of rock or of gas? # Earth Masses, # Earth radii small or large? (i.e. closer to Earth size or Jupiter size?) in outer region or inner region of solar system? hot or cold? surface T in Kelvin Lots of moons? Any other details are welcome  (eg. Does it have rings? B field?) If a planet spins in the same direction as its orbit, its spin is called “prograde”. If a planet spins in the opposite direction to its orbital motion, that spin is called “retrograde”. See contributed notes from planet teams and do your own research to supplement these powerpoint presentations. Note about T: -273 C = 0 K

Solar System Overview: Material for our contest! How do we know these things? The first 8 are planets. Note the second column.

Keplerian Rotation Curve. Solar System Overview Keplerian Rotation Curve.

Solar System Overview The density in kg/m If the density of an object is less than that of water, then it will float. The density in kg/m 1000 for water; anything less than this floats in water. 2000-3000 for rocks and 8000 for iron Note the 2nd last column. Note the density of Earth. Which planets have densities like rocks/iron? Float on water? 3

Pluto, because it is the smallest planet. Solar System Overview This classical planet would float if there was a big enough bathtub to put it in. Pluto, because it is the smallest planet. Earth, because it has so much water anyway. Europa, because it is icey. Saturn, because its density is less than water.

Solar System Overview: How do we know what we know about our solar system? Distances Diameters Masses Densities You actually have the tools to measure these things on your own.

Distances from the Sun: Solar System Overview Distances from the Sun: Radar Kepler’s Third Law (empirical) Orbits of planets are nearly circular  use Newton’s Laws for a circular orbit of radius “r”. M is mass of sun. Recall: Empirical == a law determined from observations rather than theory. Newton provided the theory. The mass of the sun is known also from the v squared equation. Note: F_inertia is the same as F_orbit. Rearrange: Need velocity to get radius.

Solar System Overview: Distances Velocity of Planets: v = distance/time Distance: The length of the path of the orbit is the circumference of a circle. Time: The time to travel the full orbit is the Period “P”. Substitute in for distance and time:

Solar System Overview: Distances Substitute v squared into the equation for radius: Just need to observe the Period to get the distance!

Solar System Overview: We have the distance! Kepler’s Third Law -- for ellipses Observe the Period! Using a in au and P in Earth years. Orbit of planet Kepler derived this empirically – that is, he didn’t have a theory about why it happened but he observed that the planets: a) travelled in ellipses “a” is the semimajor axis of an ellipse with the sun at one focus. b) there was a relationship between “a” and “P” sun a

Keplerian Rotation Curve. Solar System Overview Using P he could calculate a velocity and plot the rotation curve for the Solar System. Keplerian Rotation Curve.

2. Diameters - from lecture 4 Solar System Overview 2. Diameters - from lecture 4 Linear diameter angular diameter --------------------- = ----------------------- 2 pi * Distance 360 degrees 2 pi * Distance linear diameter = --------------------- * angular diameter 360 degrees (This could be on the test.) This can be used to measure the radius of an orbit of a moon around another planet too. We can get the distance between a planet and Earth by using step 1 to get its distance to the sun and using geometry to get the distance to the Earth. (In contemporary times, we can use radar.) Then we just need to measure the angular diameter and we have the size of the planet.

3. Masses Solar System Overview Rearrange:  use step 2 procedure. Of course this is a way to get the mass of the sun as well, using “a” = “r” and v from the orbit of a planet. There are man-made satellites that have visited Venus and Mercury. Do this with a satellite around the planet. For example the moon around the Earth. Then “r” is the Earth-Moon distance and M is the mass of the Earth. Velocity v is determined from the Period of the moon’s orbit (e.g. 1/12 of a year).

4. Density Solar System Overview And for a sphere: So (Where R is radius.) So Density is often represented by the Greek letter “rho” . Planets are almost spherical. Slightly flattened at the poles. We know the planet’s mass from step 3. and the diameter from step 2  Mass from step 3. diameter from step 2.

Solar System Overview: That is how do we know some of these values You could actually calculate these things! Note that a table like this shows us that Jupiter and the outer planets have lower density than the inner planets.

Does it revolve in the same direction as the other planets? Solar System Overview: What does the class already know about the classical planets? For each planet: Does it revolve in the same direction as the other planets? Is it primarily composed of rock or of gas? Is it small or large? (i.e. closer to Earth size or Jupiter size?) Is it in the outer region or inner region of the solar system? Is it hot or cold? Lots of moons or few? Any other details are welcome  (eg. Does it have rings?) B field? Mass and Radius only relative to Earth. Temperature only in Kelvin. If a planet spins in the same direction as its orbit, its spin is called “prograde”. If a planet spins in the opposite direction to its orbital motion, that spin is called “retrograde”. See contributed notes from planet teams and do your own research to supplement these powerpoint presentations.

Mercury Impact craters Messenger: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington Impact craters Evidence of lava flows (volcanic activity) in smooth parts Surface Temperature 100-700K

Venus: Venus Express/European Space Agency Ultraviolet Image White regions are sulfuric acid clouds. Surface Temperature 730K Revolves backwards

Earth Notable that it has a moon, life (possibly intelligent), etc. Mean Surface Temperature 290K (290 – 273 = 17C) 1 moon

Mars Mars Express/European Space Agency Hebes Chasma High Resolution Stereo Camera aboard Mars Express. Four colour filters. Mean Surface Temp 210K … about -50C around the equator. 2 moons

Jupiter New Horizons/NASA IR image. The moon in the image is IO – this is a montage. 3 IR bands  white Red Spot. Temperature at cloud tops: 124K At least 61 moons

Saturn Cassini/NASA 97K at cloud tops At least 31 moons

Uranus “True” Colour False Colour Voyager2/NASA Rolls in its orbit Mean Surface Temperature 58K At least 27 moons

Neptune Voyager2/NASA Blue since methane absorbs red light. Mean surface temperature 59K At least 13 moons.